Two key processes allow the NS/BH to accrete mass at a high rate and launch the jets during this common envelope evolution (CEE), the formation of an accretion disk and neutrino cooling by the accreted mass. The density gradients in the envelope and in the core leads to a non-axisymmetrical accretion flow where the NS/BH accretes more mass from the denser (inner to the orbit) side. The higher mass from one side results in a net specific angular momentum of the accreted gas that is sufficiently large to form an accretion disk around the compact NS/BH (e.g., [1]}, [2]}, [3]}, [4]}, [5]}, [6]}).
Efficient neutrino-cooling by the dense and hot accreted mass for accretion rates of \(\dot{M}_{\rm acc} 10^{-3} M_\odot {~\rm yr}^{-1}\)  prevents the buildup of high-pressure around the mass-accreting NS/BH and allows the high mass-accretion rate to proceed [7]}, [8]}, [9]}. The jets themselves remove some more energy from the accreting object (e.g, [10]}, [11]}, [12]}). A black hole accretor also accretes some of the energy of the accreted mass (e.g., [13]}).
